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STEREO SC/B Magnetosheath Observations

Study on O+ observations in magnetosheath during February 2007, linked to solar wind velocity and Cassini Earth flyby. Analysis of O+ density and potential sources. Potential acceleration mechanisms investigated.

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STEREO SC/B Magnetosheath Observations

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  1. STEREO SC/B Magnetosheath Observations Lynn M. Kistler Space Science Center UNH

  2. S/C B During February, 2007 Z Y X X

  3. Mass - Mass per Charge MatricesAll Energies (<80 keV) Feb 10 Feb 11 P2 P3 P1 P0 Feb 12 Feb 13 O+ O+

  4. Mass - Mass per Charge MatricesFeb 13, 2007Individual Energies 79 keV/e 59 keV/e P2 P3 P1 P0 40 keV/e 29 keV/e

  5. Density Calculation S/CA H+ (SW) S/C B H+ (Magnetosheath) S/C A Priority 3 (SW) S/C B Priority 3 (M-Sheath) S/CA Priority 3 (1-hr averages) S/C B Priority 3 (1-hr averages) (this is the O+) Feb 10 Feb 21

  6. Density Calculation S/CA H+ (SW) S/C B H+ (Magnetosheath) S/C A Priority 3 (SW) S/C B Priority 3 (M-Sheath) S/CA Priority 3 (1-hr averages) S/C B Priority 3 (1-hr averages) Mar 1 Feb 1

  7. Summary • In the dusk-side magnetosheath, we observe bursts of energetic (30-80 keV) O+ • The O+ correlates with times of high solar wind velocity. • It is observed as far as 300 Re down the tail.

  8. Cassini Earth Flyby From Doug Hamilton

  9. CASSINI/CHEMS Magnetosheath Data From Doug Hamilton

  10. From Doug Hamilton

  11. Possible Sources • Earth’s Ring Current • Energetic O+ exits the magnetosphere at the dayside magnetopause, and then gets swept up in the sheath flow • Upflowing O+ ions from the cusp. • Would they get accelerated enough • CLUSTER is located at front-side magnetopause/bow-shock - maybe it can see the source - stay tuned ...

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